We present results from the May 1997 SOHO-Ulysses quadrature, near sunspot minimum. Ulysses was at 5.1 AU, 100 north of the solar equator, and off the east limb. It was, by chance, also at the very northern edge of the streamer belt. Nevertheless, SWOOPS detected only slow, relatively smooth wind and there was no direct evidence of fast wind from the northern polar coronal hole or of mixing with fast wind. LASCO images show that the streamer belt at 10 N was narrow and sharp at the beginning and end of the two week observation interval, but broadened in the middle. A corresponding change in density, but not flow speed, occurred at Ulysses. Coronal densities derived from UVCS show that physical parameters in the lower corona are closely related to those in the solar wind, both over quiet intervals and in transient events on the limb. One small transient observed by both LASCO and UVCS is analyzed in detail.

Suess, Steven T.↗

NASA NTRS2000

The Latitudinal Distribution of Solar Wind Magnetic Holes

Using the fast latitude scan period of the Ulysses spacecraft, the occurrence of magnetic holes in the solar wind is investigated from -80 degrees to +80 degrees helio-latitude.

Solar Wind Plasma↗

NASA NTRS2000

The Solar Magnetic Field and the Solar Wind: Existence of Preferred Longitudes

UNKNOWN

Solar↗

NASA NTRS2000

The Solar Wind

Shortly before the beginning of the space age, Eugene N. Parker of the University of Chicago predicted that interplanetary space would be filled with a plasma flowing rapidly outward from the Sun.

Solar↗

NASA NTRS1999

The Solar Magnetic Field and the Solar Wind: Existence of Preferred Longitudes

Direct measurements of the solar wind and the interplanetary magnetic field acquired over more than three solar cycles both near Earth and in interplanetary space are used to search for signatures of a persistent dependence of solar wind properties on solar longitude.

solar↗

NASA NTRS1999

Ulysses Measurements of Proton Anisotropies in the Solar Wind

Explore the source record for details and available documents.

Ulysses Proton Anisotropie Solar Wind↗

NASA NTRS1999

Observation of Secondary Proton Beams by the Ulysses SWOOPS Plasma Detector

Explore the source record for details and available documents.

secondary proton beams Ulysses SWOOPS Plasma Detec↗

NASA NTRS1999

Microstructures in the Polar Solar Wind: Ulysses

UNKNOWN

Microstructures↗

NASA NTRS1999

Identification of Trailing Edge Solar Wind Stream Interfaces: A Comparison of Ulysses Plasma and Composition Measurements

In early 1992, at 13 degrees south latitude, in transit to the southern solar pole, Ulysses began to sample a recurrent high-speed solar wind stream which emanated from a coronal hole at the south pole of the Sun.

solar↗

NASA NTRS1999

Microstructures in the Polar Solar Wind: Ulysses

We find that small (10-200 rP) magnetic decreases comprise a dominant part of the polar solar wind microstructure at Ulysses distances (2.2 AU). These magnetic field dips are almost always bounded by tangential discontinuities, a feature which is not well understood at this time. Hundreds of these events have been examined in detail and a variety of types have been found. These will be described. It is speculated that these structures have been generated by perpendicular heating of ions closer to the Sun and have then been convected to distances of Ulysses. Such structures may be very important for the rapid cross- field diffusion of ions in the polar regions of the heliosphere.

Tsuruyani, Bruce T.↗

NASA NTRS1999

Time Variabilities of Solar Wind Ion Fluxes and of X-ray and EUV Emissions from Comet Hyakutake

Observations of X-ray and extreme ultraviolet (EUV) emissions from comet C/Hyakutake 1996 B2 made by the Rontgen X-ray satellite (ROSAT) and the Extreme Ultraviolet Explorer (EUVE) revealed a total X-ray luminosity of about 500 MW.

ion fluxes↗